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Spectral Properties of Xrbs in Dusty Early-Type Galaxies

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Spectral Properties of Xrbs in Dusty Early-Type Galaxies Spectral properties of XRBs in dusty early-type galaxies N. D. Vagshette, M. B. Pandge, M.K. Patil∗ School of Physical Sciences, S.R.T.M. University, Nanded-431 606 (MS), India Tel.+91-2462-229242; +91-9405938449/Fax:+91-2462-229245 Abstract We present spectral properties of a total of 996 discrete X-ray sources resolved in a sample of 23 dusty early-type galaxies selected from different environments. The combined X-ray luminosity function of all the 996 sources within the optical D25 of the sample galaxies is well described by a broken power law with a break at 2.71 1038erg s−1 and is close to × the Eddington limit for a 1.4M⊙ neutron star. Out of the 996, about 63% of the sources have their X-ray luminosities in the range between few 1037to 2.0 1039erg s−1and are like × × normal LMXBs; about 15-20% with luminosities < few 1037 erg s−1 are either super- × soft or very-soft sources; while the remainder represents ULXs, HMXBs or unrelated heavily absorbed harder sources. More XRBs have been detected in the galaxies from isolated regions while those from rich groups and clusters host very few sources. The X-ray color-color plot for these sources has enabled us to classify them as SNRs, LMXBs, HMXBs and heavily absorbed AGNs. The composite X-ray spectra of the resolved sources within D25 region of each of the galaxies are best represented by a power law with the average photon spectral index close to 1.65. The contribution of the resolved sources to the total X-ray luminosity of their host is found to vary greatly, in the sense that, in galaxies like NGC 3379 the XRB contribution is about 81% while for NGC 5846 it is only 2%. A correlation has been evidenced between the arXiv:1205.6057v2 [astro-ph.CO] 16 Jan 2013 cumulative X-ray luminosity of the resolved sources against the star formation rate and the Ks band luminosity of the target galaxies indicating their primordial origin. Keywords: galaxies: elliptical and lenticular, cD - X-rays: binaries - X-rays: galaxies 1. Introduction The X-ray emission from early-type galaxies (ETGs; ellipticals and lenticulars) has been subject of investigations and theoretical modeling ever since their detection for the first time ∗ Corresponding author Email address: [email protected] (M.K. Patil) Preprint submitted to New Astronomy February 10, 2018 with the Einstein telescope ([13]). It is now well established that X-rays from these galaxies partly originates from hot interstellar medium (ISM) and partly from a population of X-ray binaries (XRBs; see e.g. reviews by [8], [7]), with the latter component being more important for the case of X-ray faint early-type galaxies ([33]). An XRB contains either a neutron star (NS) or a black hole (BH) accreting material from a companion star. Regardless the nature of the compact object, depending on the mass of the donor star, XRBs come in two basic flavors: the high-mass X-ray binaries (HMXBs) and the low-mass X-ray binaries (LMXBs). HMXBs are predominantly powered by the stellar winds from a young massive O or B star and are mostly found in late-type galaxies. LMXBs are the long lived systems in which a Roche Lobe overflowing low mass ( 1M⊙) star is supplying material to the compact ∼ accreting object. As early-type galaxies are dominated by the old stellar populations (with age 1 Gyr), the majority of the X-ray sources in these systems are believed to be LMXBs ≥ rather than short lived ( 107 yr) high-mass objects. Thus, the population of HMXBs scales ∼ with the star-formation rate ([19]), while that of the LMXBs scales with the stellar content of the host galaxies ([16]). Traditionally, ETGs were regarded as simple structures, devoid of gas and dust. However, the classical notion of being dry, passively evolving systems have amply changed with the employment of both ground and space-based telescopes across the electromagnetic spectrum. Extensive studies conducted on the content of ISM in early-type galaxies using the multi- wavelength data have established that the ETGs hosts complex, multi-phase ISM (e.g. [1], [6],[30], [45], [18], [36], [10]). In particular, about 50-80% of the ETGs are known to host dust in a variety of morphological forms (see e.g. [18], [36], [10], [9]). Further, past studies have also demonstrated that dust in these galaxies is having external origin i.e., accreted by the system either through interaction or merger like event ([2], [17], [36], [35], [43]). Given the external origin of the dust, investigation of populations of XRBs in dusty ETGs are important to constrain the formation scenario of this class of galaxies. Therefore, a systematic study of properties of discrete sources in a relatively larger sample of dusty early-type galaxies is called for. We have an ongoing program of examining the association of multi-phase ISM in a sam- ple of dusty early type galaxies (D-ETGs) selected from different environments i.e, isolated regions, fields, groups and clusters. Analysis of high resolution multi-wavelength data on these galaxies has confirmed the spatial correspondence between the dust and the ionized gas in a large fraction of galaxies and in some cases with the X-ray emitting region too, point- 2 Table 1: Global parameters of the program galaxies Sr. Obj. Morph. z Mag Obs-ID Exp. GTI Environment No. (MB ) (ks) (ks) (1) (2) (3) (4) (5) (6) (7) (8) (9) 1 NGC 1395 E2 0.00573 10.97 799 28 22 BGG 2 NGC 1399 E1 0.00475 10.00 240 44 43 BCG 3 NGC 1404 E1 0.00649 10.95 2942 30 29 CG 4 NGC 1407 E0 0.00593 10.7 791 49 44.4 CG 5 NGC 2768 S0 0.00458 10.84 9528 65 64 FG 6 NGC 3377 E5-6 0.00222 11.24 2934 40 39.5 GG 7 NGC 3379 E1 0.00304 10.24 1587 32 30.9 FG 8 NGC 3585 E7/S0 0.00478 10.88 9506 60 59 GG 9 NGC 3607 SA(s)0 0.0032 10.82 2073 39 38.4 BGG 10 NGC 3801 S0/a 0.0111 12.96 6843 60 58.2 CG 11 NGC 3923 E7/S0 0.00580 10.88 1563 22 15.60 BGG 12 NGC 4125 E6 0.00452 10.65 2071 65 62 BGG 13 NGC 4278 E1-2 0.00217 11.20 7081 111 110 GG 14 NGC 4365 E3 0.00415 10.52 2015 41 40.4 CG 15 NGC 4374 E1 0.00354 10.09 803 29 27.8 CG 16 NGC 4473 E5 0.00749 11.16 4688 30 29.4 CG 17 NGC 4494 E1-2 0.00448 10.71 2079 25 22 GG 18 NGC 4552 E 0.00113 10.73 2072 55 53.7 CG 19 NGC 4649 E2 0.00373 9.81 8182 53 48.8 CG 20 NGC 4697 E6 0.00414 10.14 784 40 38 BGG 21 NGC 5813 E1-2 0.00658 11.45 9517 99 98.1 BGG 22 NGC 5846 E0-1 0.00572 11.05 788 30 23 BGG 23 NGC 5866 S03 0.00224 10.74 2879 34 29.7 BGG Notes: col.2 - galaxy identification; col.3 - morphological type; col.4 - redshift; col.5 - absolute magnitude in B band; col.6 - Chandra observation identification number; Col. 7 - exposure time; Col. 8 - good time interval (GTI) after light curve filtering; & Col. 9 - environments of the target galaxies; where GG: member of the group, FG: Field galaxy, CG: member of cluster, LG: member of loose group, BGG: brightest galaxy in the group, BCG: brightest cluster galaxy. 3 ing towards their common origin ([43], [34]). During this study we found that the D-ETGs also host a significant number of discrete sources whose populations and characteristics are believed to vary as a function of environment of the host galaxy. This paper presents a sys- tematic study of the spectral properties of discrete sources detected within the D25 (isophote of the 25.0 B-mag arcsec−2 brightness level; [5]) regions of the sample galaxies. In addition to this, an attempt is also made to classify these sources on the basis of their X-ray colors and also to disentangle their contribution to the total X-ray luminosity of the host. This paper is structured as follows: Section 2 describes the sample selection, X-ray observations and the steps involved in the data preparation. Results derived from this analysis are presented in Section 3, whereas Section 4 discusses some of the important results. All the distance −1 −1 dependent estimates are based on the H0 = 70 km s Mpc . 2. Observations and Data Preparation We have constructed a heterogeneous sample of 23 nearby early-type galaxies on the basis of their “dustyness”. Care was taken that the objects represent different environmental conditions i.e., isolated regions, groups and clusters. Here, we considered the objects with radial velocities 5000 km/s that were observed for at least about 20 ks by the Chandra ≤ telescope. The global properties of the target galaxies along with details of their Chandra observations are given in Table 1. Most of the target galaxies selected for the present study were observed with the ACIS-S detector, except for NGC 1395 and NGC 3607 where ACIS-I was employed. The data products on the target galaxies were uniformly processed using the Chandra In- teractive Analysis of Observations software package (CIAO) v4.2.0 and the latest calibration files provided by the Chandra X-ray data Centre (CALDB v4.3.1).
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